Homework 6, due October 27: Problems in Measuring the Universe:
|
|
- Jade Flynn
- 5 years ago
- Views:
Transcription
1 Homework 6, due October 27: Problems in Measuring the Universe: 4.2. You want to observe a star at -10 degrees declination through no more than two air masses from a telescope at 20 degrees north latitude. On the most favorable nights, how long can you observe the star? Ignoring the minor effects of atmospheric refraction, two air masses occurs at an elevation of 30 o (i.e., 1/sin(30 o ) = 2). The coordinate transformations in Section can be used to determine the range of hour angle when the source will be at greater than 30 o altitude. Solving the one giving the sine of the altitude in terms of the latitude for the observation and the declination and hour angle of the source, we have Substituting the given values yields cos h = , that is for angles < o from the meridian, the source is above 2 air masses. Converting to hour angle, this condition is met for about seven hours on a night when the source can be observed fully before and after meridian passage The first moment can be used to determine the centroid of a distribution of measurements (e.g., the measurements of an image by the pixels of an array): where the I i are the signals at positions x i. Use this approach to evaluate the impact of interpixel gaps and sampling on centroiding accuracy. Assume a Gaussian image, and that the array pixels have uniform response over 80% of their widths, but the response is only 0.9 times the central value for the outer 10% at either side. Place the image half way between the center and edge of one of the pixels and calculate the centroiding error as a function of the pixel sampling. For 1 arcsec FWHM seeing, what level of sampling is required to keep the centroiding error below 10 mas? This problem requires constructing a one-dimensional model of the signal and response to it, and then making the calculations based on the model. The answer is that the pixels need to be no larger than 0.98 arcsec. Of course, other considerations (less than infinite signal to noise, seeing fluctuations, etc.) would make the required pixel size smaller in realistic situations.
2 5.1 The list below gives Johnson system photometry of a number of stars at J and K. Kidger and Martin- Luis (2003) report JHK observations of bright stars, including the ones listed below. Look up these stars in the paper and compute the transformations to put the Johnson J, K photometry on the same basis as the Kidger and Martin-Luis J, K photometry. Name Type J K Name type J K HR 33 F5V HR 5107 A3V HR 509 G8V HR 5854 K2IIIb HR 1256 K0III HR 5947 K2III HR 1286 K1II-III HR 6623 G5IV HR 1791 B7III HR 6698 G9III HR 1907 K0IIIb HR 6705 K5III HR 1963 K1III HR 6707 F2II HR 2077 K0III HR 7236 B9Vn HR 2427 K3Iab HR 7525 K3II HR 2560 G5III-IV HR 7557 A7V HR 3003 K4III HR 7615 K0III HR 4335 K1III HR 7949 K0III HR 4377 K3III HR 8143 B9Iab HR 4608 G8IIIa HR 8632 K2III HR 4737 K1III HR 8905 F8IV HR 4983 F9.5V The figure below is a plot of the difference in J (Johnson) -J(Kidger/Martin-Luis) vs. J-K. Immediately one sees two discordant points, which since one was high and the other low, I threw out (and assigned hollow symbols). They might be bad measurements, or maybe variable stars. The line is a linear regression fit to the remaining points. The rms scatter around the line is 0.022, so it is a good fit.
3 The same thing can be done at K, see next figure. Again, I got rid of the high and low outliers (in this case I did a preliminary fit to be sure I knew which one was the high outlier - the point to the upper left was also a candidate but the fit showed it was not so bad). The linear regression fit to the remaining points has rms scatter of 0.024, again showing the fit is good. What is really surprising is that the Johnson photometry is so accurate.
4 My results are J Johnson = JKM L (J K)KM L KJohnson = KKM L (J K)KM L 5.3. Assume you have a somewhat idealized J-band system with spectral response of 0.8 from 1.15 through 1.35 m and zero outside this range. What is the effective (mean) wavelength? What is the nominal (IRAS definition) wavelength? Assume your standard star has a Rayleigh Jeans spectrum across the J filter. Using the mean wavelength, compute the bandpass correction relative to the standard for the ultraluminous galaxy spectrum of d with in m The mean (or effective) wavelength of the filter is The nominal wavelength is the same expression with an extra factor of λ in both integrals; 1.253μm. To compute the bandpass correction, assume that the standard is Rayleigh-Jeans, i.e., with a spectrum
5 going as λ -4, and that it is normalized to 1 at λ 0. Convolve with the filter and integrate. I get For the galaxy, I again normalize to 1 at 1.25 m and then convolve with the filter and integrate. I get Therefore, if the galaxy had the same flux density as the star at the filter effective wavelength, we would have gotten a smaller signal from it by the ratio / = Without the band pass correction, if we had gotten the same signals we would have thought that they had the same flux densities at the effective wavelength. To correct our error, we need to take the flux density we got for the galaxy under this assumption and increase it by the factor 1/ =
6 5.8 You have the following set of measurements, obtained from a telescope at 32 degrees north latitude: Determine m V for star 3. Hint: if you use the appropriate units, you can determine the air mass correction from a linear fit. Star m V Dec HA DU o -3.5 hours hours hours o -2.1 hours hours o 1.4 hours We use equation (4.3) to compute the air masses for each observation: star 1; 1.369, 1.120, and 1.826; star 2; 1.205, 1.683; star 3; We can plot log(du) vs. airmass (equation (5.10) suggests this approach) and fit the signals for stars 1 and 2 requiring the same slope for the two stars. This yields log(du) = * (air mass) for star 1 and log(du) = * (air mass) for star 2. At one airmass, star 1 then would have a signal of log(du) = , or DU = At one airmass, star 2 similarly would have DU, and star 3 would have DU at one airmass (for the latter, we take (am-1)*( ) and apply the resulting correction to the log of the observed DU). Relative to star 1, star 3 is then 2.5*log(1693/532.5) = magnitudes fainter, or at magnitude Relative to star 2, star 3 is 2.5*log(532.5/235.3) = 0.89 magnitudes brighter, or at magnitude We can take the average as our best estimate, You can also use the given magnitudes of the two stars to put them on the same scale to determine the airmass correction, although that depends on the magnitudes being accurate and is a bit more risky than the method used above.
Selecting an Observing Target
Chapter 2: Selecting an Observing Target Selection Criteria There are several factors that must be considered when selecting a target to observe: Is the target visible from Winnipeg? For what dates is
More informationAS750 Observational Astronomy
Lecture 9 0) Poisson! (quantum limitation) 1) Diffraction limit 2) Detection (aperture) limit a)simple case b)more realistic case 3) Atmosphere 2) Aperture limit (More realistic case) Aperture has m pixels
More informationTECHNICAL REPORT. Doc #: Date: Rev: JWST-STScI , SM-12 August 31, Authors: Karl Gordon, Ralph Bohlin. Phone:
When there is a discrepancy between the information in this technical report and information in JDox, assume JDox is correct. TECHNICAL REPORT Title: Title: JWST Absolute Flux Calibration II: Expanded
More informationAstronomy 203 practice final examination
Astronomy 203 practice final examination Fall 1999 If this were a real, in-class examination, you would be reminded here of the exam rules, which are as follows: You may consult only one page of formulas
More informationATMOS Modèle numérique d'atmosphère
Jihane Moultaka LATT Observatoire Midi Pyrénées Goal : Simulate the effect of Atmosphere on the ideal (simulated) data cube Use : Produce the most realistic data in order to Prepare the instrument Determine
More informationESO Phase 3 Data Release Description. Data Collection ATLASGAL Release Number 1 Data Provider
ESO Phase 3 Data Release Description Data Collection ATLASGAL Release Number 1 Data Provider Frederic Schuller, K. Immer, Y. Contreras, T. Csengeri, J. S. Urquhart Date 19.01.2016 Abstract The APEX Telescope
More informationProgress Towards an Absolute Calibration of Lunar Irradiance at Reflected Solar Wavelengths
Progress Towards an Absolute Calibration of Lunar Irradiance at Reflected Solar Wavelengths Claire Cramer, Steve Brown, Keith Lykke, John Woodward (NIST) Tom Stone (USGS) Motivation for using the Moon
More informationPoint Spread Functions. Aperture Photometry. Obs Tech Obs Tech 26 Sep 2017
Point Spread Functions & Aperture Photometry Obs Tech Obs Tech 26 Sep 2017 Point Spread Functions (PSFs) Stars are far away (typically d >> 3x10 15 km) Stars are relatively small (D ~ 10 6 km) Angular
More informationHelping Henrietta Leavitt Measure Cepheid Variables
Name Homework number 6: Due October Astronomy 70B Profs. Rieke Helping Henrietta Leavitt Measure Cepheid Variables Ms. Henrietta Leavitt has invited you to join her at Harvard College Observatory to look
More informationGeostationary Satellites and Astrophotography
Geostationary Satellites and Astrophotography By Clay S. Turner 11/14/08 Introduction When I first started doing astrophotography last January, it was only natural to take pictures of some of Orion s deep
More informationLecture 8. October 25, 2017 Lab 5
Lecture 8 October 25, 2017 Lab 5 News Lab 2 & 3 Handed back next week (I hope). Lab 4 Due today Lab 5 (Transiting Exoplanets) Handed out and observing will start Friday. Due November 8 (or later) Stellar
More informationYou, too, can make useful and beautiful astronomical images at Mees: Lesson 3
You, too, can make useful and beautiful astronomical images at Mees: Lesson 3 Calibration and data reduction Useful references, besides Lessons 1 and 2: The AST 142 Projects manual: http://www.pas.rochester.edu/~dmw/ast142/projects/project.pdf
More informationChapter 5: Telescopes
Chapter 5: Telescopes You don t have to know different types of reflecting and refracting telescopes. Why build bigger and bigger telescopes? There are a few reasons. The first is: Light-gathering power:
More informationFlux Units and Line Lists
APPENDIX 2 Flux Units and Line Lists In This Appendix... Infrared Flux Units / 255 Formulae / 258 Look-up Tables / 259 Examples / 266 Infrared Line Lists / 266 In this chapter we provide a variety of background
More informationDOME C AS A SETTING FOR THE PERMANENT ALL SKY SURVEY (PASS)
Title : will be set by the publisher Editors : will be set by the publisher EAS Publications Series, Vol.?, 2005 DOME C AS A SETTING FOR THE PERMANENT ALL SKY SURVEY (PASS) H.J. Deeg, J.A. Belmonte, R.
More informationFIRST carrier spacecraft
FIRST carrier spacecraft Height 9 m Width 4.5 m Launch mass 3300 kg Power 1 kw Launch vehicle Ariane 5 Orbit Lissajous around L2 Science data rate 100 kbps Telescope diametre 3.5 m Telescope WFE 10 µm
More informationsummary of last lecture
radiation specific intensity flux density bolometric flux summary of last lecture Js 1 m 2 Hz 1 sr 1 Js 1 m 2 Hz 1 Js 1 m 2 blackbody radiation Planck function(s) Wien s Law λ max T = 2898 µm K Js 1 m
More informationEXPOSURE TIME ESTIMATION
ASTR 511/O Connell Lec 12 1 EXPOSURE TIME ESTIMATION An essential part of planning any observation is to estimate the total exposure time needed to satisfy your scientific goal. General considerations
More informationOPTICAL PHOTOMETRY. Observational Astronomy (2011) 1
OPTICAL PHOTOMETRY Observational Astronomy (2011) 1 The optical photons coming from an astronomical object (star, galaxy, quasar, etc) can be registered in the pixels of a frame (or image). Using a ground-based
More informationThe in-orbit wavelength calibration of the WFC G800L grism
The in-orbit wavelength calibration of the WFC G800L grism A. Pasquali, N. Pirzkal, J.R. Walsh March 5, 2003 ABSTRACT We present the G800L grism spectra of the Wolf-Rayet stars WR45 and WR96 acquired with
More informationTransiting Exoplanet in the Near Infra-red for the XO-3 System
Transiting Exoplanet in the Near Infra-red for the XO-3 System Nathaniel Rodriguez August 26, 2009 Abstract Our research this summer focused on determining if sufficient precision could be gained from
More informationACS CCDs UV and narrowband filters red leak check
Instrument Science Report ACS 2007-03 ACS CCDs UV and narrowband filters red leak check Marco Chiaberge and Marco Sirianni May 01, 2007 ABSTRACT We present results of the observations of the star 15 Mon,
More information5. A particular star has an angle of parallax of 0.2 arcsecond. What is the distance to this star? A) 50 pc B) 2 pc C) 5 pc D) 0.
Name: Date: 1. How far away is the nearest star beyond the Sun, in parsecs? A) between 1 and 2 pc B) about 12 pc C) about 4 pc D) between 1/2 and 1 pc 2. Parallax of a nearby star is used to estimate its
More informationAy Fall 2012 Imaging and Photometry Part I
Ay 122 - Fall 2012 Imaging and Photometry Part I (Many slides today c/o Mike Bolte, UCSC) Imaging and Photometry Now essentially always done with imaging arrays (e.g., CCDs); it used to be with single-channel
More informationAtmospheric Extinction
Atmospheric Extinction Calibrating stellar photometry requires correction for loss of light passing through the atmosphere. Atmospheric Rayleigh and aerosol scattering preferentially redirects blue light
More informationSatellite Type Estination from Ground-based Photometric Observation
Satellite Type Estination from Ground-based Photometric Observation Takao Endo, HItomi Ono, Jiro Suzuki and Toshiyuki Ando Mitsubishi Electric Corporation, Information Technology R&D Center Takashi Takanezawa
More informationChapter 6: Transforming your data
Why is transformation necessary? Chapter 6: Transforming your data The AAVSO International Database is composed of data collected from many different observers, at different times, from around the globe.
More informationObservingwith a LISA spectrograph. David Boyd BAAVSS, AAVSO, CBA
Observingwith a LISA spectrograph David Boyd BAAVSS, AAVSO, CBA For me, the appeal of spectroscopy is in its scientific potential Photometry reveals changes in a star s brightness R Scutum Spectroscopy
More informationData Processing in DES
Data Processing in DES Brian Yanny Oct 28, 2016 http://data.darkenergysurvey.org/fnalmisc/talk/detrend.p Basic Signal-to-Noise calculation in astronomy: Assuming a perfect atmosphere (fixed PSF of p arcsec
More informationPan-Planets. A Search for Transiting Planets Around Cool stars. J. Koppenhoefer, Th. Henning and the Pan-PlanetS Team
Pan-Planets A Search for Transiting Planets Around Cool stars J. Koppenhoefer, Th. Henning and the Pan-PlanetS Team Pan-STARRS 1: 1.8m prototype telescope operated on Haleakala/Hawaii consortium of few
More informationThe Australia Telescope. The Australia Telescope National Facility. Why is it a National Facility? Who uses the AT? Ray Norris CSIRO ATNF
The Australia Telescope National Facility The Australia Telescope Ray Norris CSIRO ATNF Why is it a National Facility? Funded by the federal government (through CSIRO) Provides radio-astronomical facilities
More information3 Effects of the earth s atmosphere
Astr 535 Class Notes Fall 2017 29 3 Effects of the earth s atmosphere The earth s atmosphere has several different effects: it emits light, it absorbs light, it shifts the apparent direction of incoming
More informationLecture 11: SDSS Sources at Other Wavelengths: From X rays to radio. Astr 598: Astronomy with SDSS
Astr 598: Astronomy with SDSS Spring Quarter 4, University of Washington, Željko Ivezić Lecture : SDSS Sources at Other Wavelengths: From X rays to radio Large Surveys at Many Wavelengths SDSS: UV-IR five-band
More informationLAMOST Sky Survey --Site limitations and survey planning
LAMOST Sky Survey --Site limitations and survey planning Chao Liu, Licai Deng National Astronomical Observatories, CAS Heidi Newberg Rensselaer Polytechnic Institute Overview Site limitations that strictly
More informationCounting Photons to Calibrate a Photometer for Stellar Intensity Interferometry
Counting Photons to Calibrate a Photometer for Stellar Intensity Interferometry A Senior Project Presented to the Department of Physics California Polytechnic State University, San Luis Obispo In Partial
More informationTheoretical Examination
Page 1 of (T1) True or False Determine if each of the following statements is True or False. In the Summary Answersheet, tick the correct answer (TRUE / FALSE) for each statement. No justifications are
More informationImaging Capability of the LWA Phase II
1 Introduction Imaging Capability of the LWA Phase II Aaron Cohen Naval Research Laboratory, Code 7213, Washington, DC 2375 aaron.cohen@nrl.navy.mil December 2, 24 The LWA Phase I will consist of a single
More informationScience Update SBAG July, Andrew Cheng (JHU/APL) Karl Hibbitts (JHU/APL) Eliot Young (SwRI)
Science Update SBAG July, 2014 Andrew Cheng (JHU/APL) Karl Hibbitts (JHU/APL) Eliot Young (SwRI) Overview BOPPS science objectives BIRC calibration results UVVis update Science operations 4/23/14 2 BOPPS
More informationIvan Valtchanov Herschel Science Centre European Space Astronomy Centre (ESAC) ESA. ESAC,20-21 Sep 2007 Ivan Valtchanov, Herschel Science Centre
SPIRE Observing Strategies Ivan Valtchanov Herschel Science Centre European Space Astronomy Centre (ESAC) ESA Outline SPIRE quick overview Observing with SPIRE Astronomical Observation Templates (AOT)
More informationToday in Astronomy 142: observations of stars
Today in Astronomy 142: observations of stars What do we know about individual stars?! Determination of stellar luminosity from measured flux and distance Magnitudes! Determination of stellar surface temperature
More informationDirect imaging of extra-solar planets
Chapter 6 Direct imaging of extra-solar planets Direct imaging for extra-solar planets means that emission from the planet can be spatially resolved from the emission of the bright central star The two
More informationWHAT PHOTOMETRIC PRECISION CAN I ACHIEVE? DAVID BOYD
WHAT PHOTOMETRIC PRECISION CAN I ACHIEVE? DAVID BOYD If you start using a CCD camera to carry out photometry on variable stars, this is a question that sooner or later you will ask yourself. Prompted by
More informationAdvanced Image Cleaning
Introduction Algorithms Experiments Results Conclusion References CTA Consortium Meeting Jérémie DECOCK October 25, 216 Introduction Algorithms Experiments Results Conclusion References Introduction 2
More informationAtoms and Spectra October 8th, 2013
Atoms and Spectra October 8th, 2013 Announcements Second writing assignment due two weeks from today (again, on a news item of your choice). Be sure to make plans to visit one of the open observing nights
More informationAstronomy 15 - Problem Set Number 4
Astronomy 15 - Problem Set Number 4 1) Suppose one were to observe a star for parallax with a telescope of 15 meters focal length. Suppose the pixels of the CCD are 24 microns in size (1 micron = 10 6
More informationThe verification of the MASS spectral response
The verification of the MASS spectral response Victor Kornilov September 14, 2006 Introduction The paper 1 shows that the weighting functions (WF) used for turbulence profile restoration from the scintillation
More informationPhotographing the Moon and the ISS. By Thierry Legault
Photographing the Moon and the ISS By Thierry Legault Photographing the whole Moon: basics Needs a DSLR at prime focus of the telescope The field of view depends on the telescope FL and the size S of the
More informationOn the calibration of WFCAM data from 2MASS
On the calibration of WFCAM data from 2MASS Authors: Simon Hodgkin, Mike Irwin Draft: September 28 th 2006 Modifications: ID: VDF-TRE-IOA-00011-0000* 1 Introduction The requirement on VDFS is to photometrically
More informationInfrared standards for ISO
ASTRONOMY & ASTROPHYSICS FEBRUARY II 1998, PAGE 207 SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 128, 207-219 (1998) Infrared standards for ISO I. A new calibration of mid infrared photometry P.L.
More informationFluxes. 1 March 2016
Fluxes 1 March 2016 intrinsic luminosity L = energy emi5ed per second (erg/s) intrinsic luminosity L = energy emi5ed per second (erg/s) flux F = energy received per unit area F = L / 4π d 2 (erg/s/cm 2
More informationPhotometric Systems. Neil Phillips 08 April Introduction 1. 2 Magnitudes and Colours 2
Photometric Systems Neil Phillips 8 April 28 Contents 1 Introduction 1 2 Magnitudes and Colours 2 3 Performing photometry 2 3.1 The System Response R λ....................................
More informationIN REPORT: Plate Scale and FOV of CCD for Each Telescope using Albireo Stars
USE ASTROIMAGEJ NOT AIP4WIN To download ALL the public data from Canvas, go to Files, then click the 3 dots next to the Public Data Folder and click Download. It will download all the files at once. 6.1
More informationPhotometric Products. Robert Lupton, Princeton University LSST Pipeline/Calibration Scientist PST/SAC PST/SAC,
Photometric Products Robert Lupton, Princeton University LSST Pipeline/Calibration Scientist PST/SAC 2018-02-27 PST/SAC, 2018-02-27 LSST2017 Tucson, AZ August 14-18, 2017 1 Outline Photometry Point Sources
More informationLarge Area Imaging Survey of Near-Infrared Sky with Korean Compact Space Telescopes
Large Area Imaging Survey of Near-Infrared Sky with Korean Compact Space Telescopes Science & Technology Satellite Series (KARI) (2000 ~ 2013. 02) 1 st Satellite: FIMS (Far-ultraviolet IMaging Spectrograph)
More information70µm Warm Campaign 10K Sensitivity Tests D. Frayer, A. Noriega-Crespo, S. Wachter, & D. Fadda (MIPS-IST) 2005-Jun-16, Version 1.
1 70µm Warm Campaign 10K Sensitivity Tests D. Frayer, A. Noriega-Crespo, S. Wachter, & D. Fadda (MIPS-IST) 2005-Jun-16, Version 1. Abstract Data were recently taken to quantify the 70µm sensitivity and
More informationThe SKYGRID Project A Calibration Star Catalog for New Sensors. Stephen A. Gregory Boeing LTS. Tamara E. Payne Boeing LTS. John L. Africano Boeing LTS
The SKYGRID Project A Calibration Star Catalog for New Sensors Stephen A. Gregory Boeing LTS Tamara E. Payne Boeing LTS John L. Africano Boeing LTS Paul Kervin Air Force Research Laboratory POSTER SESSION
More informationModern Navigation. Thomas Herring
12.215 Modern Navigation Thomas Herring Review of last Class Review of linear Algebra. Class will be based on the book Linear Algebra, Geodesy, and GPS, G. Strang and K. Borre, Wellesley-Cambridge Press,
More informationLab 4 Radial Velocity Determination of Membership in Open Clusters
Lab 4 Radial Velocity Determination of Membership in Open Clusters Sean Lockwood 1, Dipesh Bhattarai 2, Neil Lender 3 December 2, 2007 Abstract We used the Doppler velocity of 29 stars in the open clusters
More informationRecent Observations of Supernova Remnants
1 Recent Observations of Supernova Remnants with VERITAS Tülün Ergin (U. of Massachusetts Amherst, MA) on behalf of the VERITAS Collaboration (http://veritas.sao.arizona.edu) 2 Contents Supernova Remnants
More informationThe HII Regions of Sextans A
Publications of the Astronomical Society of the Pacific 6: 765-769, 1994 July The HII Regions of Sextans A Paul Hodge 1 Astronomy Department, University of Washington, Seattle, Washington 98195 Electronic
More informationSpeckles and adaptive optics
Chapter 9 Speckles and adaptive optics A better understanding of the atmospheric seeing and the properties of speckles is important for finding techniques to reduce the disturbing effects or to correct
More informationHostless Supernovae Anna Marlatt Advisor: Dr. David Cinabro
Hostless Supernovae Anna Marlatt Advisor: Dr. David Cinabro 1 Abstract In this paper, I discuss hostless supernovae. These are described as supernovae that do not have a host galaxy. The sample that we
More informationStatistical Properties of Geosynchronous Satellite Photometry
Statistical Properties of Geosynchronous Satellite Photometry Tamara E. Payne Applied Optimization Inc. Abstract This paper presents the general properties of a set of observations of satellites in Geosynchronous
More informationStellar Photometry: II. Transforming. Ast 401/Phy 580 Fall 2015
Stellar Photometry: II. Transforming Ast 401/Phy 580 Fall 2015 Summary We ve learned how to measure instrumental magnitudes for a star using aperture photometry or PSF-fitting: (a) Add up all of the counts
More informationWelcome to Astronomy 402/602
Welcome to Astronomy 402/602 Introductions Syllabus Telescope proposal Coordinate Systems (Lecture) Coordinate System Exercise Light (Lecture) Telescopes (Lecture) Syllabus Course goals Course expectations
More informationPACS_S Flux Calibration Concept
PACS_S Flux Calibration Concept Original concept: point source on central spaxel, sum of signals from all spaxels must add up to total flux of source At some point, replaced by (adopted) "point source
More informationHigh Signal-to-Noise, Differential NICMOS Spectrophotometry
Instrument Science Report NICMOS 2003-001 High Signal-to-Noise, Differential NICMOS Spectrophotometry R.L. Gilliland, S. Arribas January 7, 2003 ABSTRACT We report analysis for NICMOS CAL/9642, High S/N
More informationLecture #15: Plan. Telescopes (cont d) Effects of Earth s Atmosphere Extrasolar planets = Exoplanets
Lecture #15: Plan Telescopes (cont d) Effects of Earth s Atmosphere Extrasolar planets = Exoplanets Resolving Power (review) The bigger the size of the telescope, the better it is at discerning fine details
More informationUnderstanding Positional Astronomy Part 2 Celestial Co-ordinates Difficulty: Intermediate
Exercise: Understanding Positional Astronomy Part 2 Celestial Co-ordinates Difficulty: Intermediate Objectives In Part 1 you learned about Celestial Sphere and how the stars appear to move across the night
More informationImage Processing in Astronomy: Current Practice & Challenges Going Forward
Image Processing in Astronomy: Current Practice & Challenges Going Forward Mario Juric University of Washington With thanks to Andy Connolly, Robert Lupton, Ian Sullivan, David Reiss, and the LSST DM Team
More informationThe HR Diagram: A Laboratory Exercise
Pisgah Astronomical Research Institute 2009 The HR Diagram: A Laboratory Exercise The HR Diagram Lab gives students the opportunity to construct an HR Diagram based on their own classifications of 119
More informationSMA Mosaic Image Simulations
l To: Files From: Douglas Wood Date: Monday, July 23, 1990 Subject: SMA Technical Memo #23 SMA Mosaic mage Simulations Abstract This memo presents some preliminary results of SMA image simulations using
More informationRadiation from planets
Chapter 4 Radiation from planets We consider first basic, mostly photometric radiation parameters for solar system planets which can be easily compared with existing or future observations of extra-solar
More informationChapter 10: Unresolved Stellar Populations
Chapter 10: Unresolved Stellar Populations We now consider the case when individual stars are not resolved. So we need to use photometric and spectroscopic observations of integrated magnitudes, colors
More informationOutline. Mm-Wave Interferometry. Why do we care about mm/submm? Star-forming galaxies in the early universe. Dust emission in our Galaxy
Outline 2 Mm-Wave Interferometry Debra Shepherd & Claire Chandler Why a special lecture on mm interferometry? Everything about interferometry is more difficult at high frequencies Some problems are unique
More informationKeck Adaptive Optics Note #385. Feasibility of LGS AO observations in the vicinity of Jupiter. Stephan Kellner and Marcos van Dam
Keck Adaptive Optics Note #385 Feasibility of LGS AO observations in the vicinity of Jupiter Stephan Kellner and Marcos van Dam Version 2: 25 July 2006 1 Introduction It has been proposed by Imke De Pater
More informationMeasuring stellar distances.
Measuring stellar distances This method can be used to measure distances up to 100pc Some new technology allows measuring distances up to 200pc using this method p= 1/d Stellar Parallax.htm This method
More informationEarly-Science call for observing time with SAM-FP
Early-Science call for observing time with SAM-FP 1. General description SOAR is opening a call for proposals for early-science with SAM-FP in 2016B, for 4 nights (September 29 October 2, 2016). SAM-FP
More informationSimulation of UV-VIS observations
Simulation of UV-VIS observations Hitoshi Irie (JAMSTEC) Here we perform radiative transfer calculations for the UV-VIS region. In addition to radiance spectra at a geostationary (GEO) orbit, air mass
More informationLab 4: Differential Photometry of an Extrasolar Planetary Transit
Lab 4: Differential Photometry of an Extrasolar Planetary Transit Neil Lender 1, Dipesh Bhattarai 2, Sean Lockwood 3 December 3, 2007 Abstract An upward change in brightness of 3.97 ± 0.29 millimags in
More informationUltimate Events. Galaxy clustering in ever deeper surveys. Models of universe and its fates
ASTR 1040 Accel Astro: Stars & Galaxies Ultimate Events Prof. Juri Toomre TA: Nicholas Nelson Lecture 30 Thur 28 Apr 2011 zeus.colorado.edu/astr1040-toomre toomre Allen Telescope Array Review current big
More informationE-ELT Spectroscopic ETC: Detailed Description
E-ELT Spectroscopic ETC: Detailed Description Jochen Liske Based on a document originally written by Pascal Ballester, Andrés Jordán, Markus Kissler- Patig & Jakob Vinther. 1. Preliminaries As of Jan 2008
More information1 Lecture, 2 September 1999
1 Lecture, 2 September 1999 1.1 Observational astronomy Virtually all of our knowledge of astronomical objects was gained by observation of their light. We know how to make many kinds of detailed measurements
More informationName Class Date. For each pair of terms, explain how the meanings of the terms differ.
Skills Worksheet Chapter Review USING KEY TERMS 1. Use each of the following terms in a separate sentence: year, month, day, astronomy, electromagnetic spectrum, constellation, and altitude. For each pair
More informationSearching for Other Worlds
Searching for Other Worlds Lecture 32 1 In-Class Question What is the Greenhouse effect? a) Optical light from the Sun is reflected into space while infrared light passes through the atmosphere and heats
More informationCommissioning of the Hanle Autoguider
Commissioning of the Hanle Autoguider Copenhagen University Observatory Edited November 10, 2005 Figure 1: First light image for the Hanle autoguider, obtained on September 17, 2005. A 5 second exposure
More informationLecture 12: Distances to stars. Astronomy 111
Lecture 12: Distances to stars Astronomy 111 Why are distances important? Distances are necessary for estimating: Total energy released by an object (Luminosity) Masses of objects from orbital motions
More information9. Evolution with redshift - z > 1.5. Selection in the rest-frame UV
11-5-10see http://www.strw.leidenuniv.nl/ franx/college/galaxies10 10-c09-1 11-5-10see http://www.strw.leidenuniv.nl/ franx/college/galaxies10 10-c09-2 9. Evolution with redshift - z > 1.5 Selection in
More informationQuestion Details UNCAstro101L1 5.IL.001. [ ]
Lab 5: Distance Ladder II: Standard Candles (T) (2628698) Due: Fri Nov 7 2014 12:00 PM EST Question 1 Instructions Lab 5: The Cosmic Distance Ladder II: Standard Candles Read the lab before attending lab.
More informationOverview of comparison data presented
SUPPLEMENTARY INFORMATION doi:10.1038/nature09452 Overview of comparison data presented In Figure 2, we compare our results with four other data sets chosen to reflect much of the universe in which galaxy
More informationCCD astrometry and UBV photometry of visual binaries
ASTRONOMY & ASTROPHYSICS JUNE I 1998, PAGE 299 SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 130, 299 304 (1998) CCD astrometry and UBV photometry of visual binaries II. Visual double stars with mainly
More informationA Stellar Spectra 3. Stars shine at night (during the day too!). A star is a self-luminous sphere of gas. Stars are held together by gravity.
Stellar Spectra Relativity and Astrophysics Lecture 12 Terry Herter Outline What is a star? Stellar Spectra Kirchhoff s Laws Spectral Classification Spectral Types: O B A F G K M L T Stellar Photometry
More informationWFC3/UVIS Photometric Transformations
Instrument Science Report WFC3 2014-016 WFC3/UVIS Photometric Transformations Kailash Sahu, Susana Deustua and Elena Sabbi January 05, 2017 ABSTRACT We provide photometric transformation coefficients for
More informationDelivery of a new ACS SBC throughput curve for Synphot
Delivery of a new ACS SBC throughput curve for Synphot Francesca R. Boffi, M. Sirianni, R. A. Lucas, N. R. Walborn, C. R. Proffitt April 18, 2008 ABSTRACT On November 12th, 2007 a new ACS SBC throughput
More informationThe Optical Microvariability and Spectral Changes of the BL Lacertae Object S
J. Astrophys. Astr. (2011) 32, 97 103 c Indian Academy of Sciences The Optical Microvariability and Spectral Changes of the BL Lacertae Object S5 0716+714 H. Poon 1,, J.H.Fan 2 & J.N.Fu 1 1 Astronomy Department,
More informationSky demonstration of potential for ground layer adaptive optics correction
Sky demonstration of potential for ground layer adaptive optics correction Christoph J. Baranec, Michael Lloyd-Hart, Johanan L. Codona, N. Mark Milton Center for Astronomical Adaptive Optics, Steward Observatory,
More informationAstronomical Instrumentation and Statistics
Astronomical Instrumentation and Statistics This figure is a nice summary of the impact of new technology on new discoveries. It plots the time the necessary technology was available prior to making a
More informationImaging with SPIRIT Exposure Guide
Imaging with SPIRIT Exposure Guide SPIRIT optical telescopes utilise extremely sensitive cameras to record the light from distant astronomical objects. Even so, exposures of several seconds up to a few
More informationThe complex gravitational lens system B
Mon. Not. R. Astron. Soc. 301, 310 314 (1998) The complex gravitational lens system B1933+503 C. M. Sykes, 1 I. W. A. Browne, 1 N. J. Jackson, 1 D. R. Marlow, 1 S. Nair, 1 P. N. Wilkinson, 1 R. D. Blandford,
More informationKepler photometric accuracy with degraded attitude control
Kepler photometric accuracy with degraded attitude control Hans Kjeldsen, Torben Arentoft and Jørgen Christensen-Dalsgaard KASOC, Stellar Astrophysics Centre, Aarhus University, Denmark - 25 July 2013
More information